Extended Data Fig. 3: Identification efficiency test in the presence of precession effects.
From: An interference-based method for the detection of strongly lensed gravitational waves
This figure shows the match between the maximum likelihood waveform from cWB and the posterior results from Bilby, as a function of GW SNR. The light grey (dark grey) shaded area represents the lowest match values between cWB and Bilby for unlensed events with (without) precession effects. The blue pentagrams (indicating the mean value) with black error bars (representing the 90% confidence interval) depict the match results for SLGWs. This plot employs a cut-off at a detector-frame chirp mass of \({{\mathcal{M}}}_{z}\ge 20M\odot\).
